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HAYABUSA is the first spacecraft ever to land on and lift off from anycelestial body other than the moon. The mission, which returned asteroidsamples to the Earth while overcoming various technical hurdles, ended on June13, 2010, with the planned atmospheric re-entry. In order to safely deliver thesample return capsule, the HAYABUSA spacecraft ended its 7-year journey in abrilliant "artificial fireball" over the Australian desert. Spectroscopicobservation was carried out in the near-ultraviolet and visible wavelengthsbetween 3000 and 7500 \AA at 3 - 20 \AA resolution. Approximately 100 atomiclines such as Fe I, Mg I, Na I, Al I, Cr I, Mn I, Ni I, Ti I, Li I, Zn I, O I,and N I were identified from the spacecraft. Exotic atoms such as Cu I, Mo I,Xe I and Hg I were also detected. A strong Li I line (6708 \AA) at a height of~55 km originated from the onboard Li-Ion batteries. The FeO molecule bands ata height of ~63 km were probably formed in the wake of the spacecraft. Theeffective excitation temperature as determined from the atomic lines variedfrom 4500 K to 6000 K. The observed number density of Fe I was about 10 timesmore abundant than Mg I after the spacecraft explosion. N2+(1-) bands from ashock layer and CN violet bands from the sample return capsule's ablating heatshield were dominant molecular bands in the near-ultraviolet region of 3000 -4000 \AA. OH(A-X) band was likely to exist around 3092 \AA. A strong shocklayer from the HAYABUSA spacecraft was rapidly formed at heights between 93 kmand 83 km, which was confirmed by detection of N2+(1-) bands with a vibrationtemperature of ~13000 K. Gray-body temperature of the capsule at a height of~42 km was estimated to be ~2437 K which is matched to a theoreticalprediction. The final message of the HAYABUSA spacecraft and its sample returncapsule are discussed through our spectroscopy.

Near-Ultraviolet and Visible Spectroscopy of HAYABUSA Spacecraft Re-entry